Transcript 슬라이드 1

Tai Hyun Yoon (Korea Univ.)
on behalf of the Korean Gravitational-Wave Group (KGWG)
The LCGT Face-To-Face Meeting, ICRR
August 3-5, 2011
Outline
I. Korean Gravitational-Wave Group (KGWG)
II. Proposed Works
1.
2.
3.
Experimental Involvement
Data Analysis
Astrophysical Research
III. Facilities
IV. Human Resources
V. Summary
http://kgwg.nims.re.kr
The KGWG and The LCGT
Motivations:
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KGWG members have strong interests on
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Experimental challenges of LCGT (T. H. Yoon, Korea Univ.)
New Korea-Japan Joint Research Project has been started (T. H. Yoon & S.
Kawamura): July 1, 2011 – Jun 30, 2013
Data analysis of gravitational wave detectors (H. M. Lee, Seoul Nat. Univ)
Relativistic astrophysics, compact objects, and gravitational waves (M. van Putten,
KIAS)
KGWG has experiences in LIGO/Virgo data analysis as well as large
observational and experimental data
Korea will have excellent observational facilities (e.g. Korea Microlensing
Telescope Network: KMT-Net) for research related to transient searches
KGWG can provide
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Manpower for experiment, data analysis and management
Powerful computing resources for the LCGT data analysis
Astrophysical research opportunities related to LCGT experiments
seismometer
double
magnetic
shields
2D-MOT
87Rb
L2 : repumper / Raman 1
L3 : cooling / Raman 2
σ+
σ-
Raman collimator
with adjustable /4
West 3D-MOT beam
East 3DMOT
beam
3D-MOT
detection
detection
σ-
σ+
λ/4
retro-reflection
mirror
isolation
platform
LCGT Input Optics
Isolator for backward light
Mode Cleaner
ETMy
Pre Mode Cleaner
Intensity stabilization
ITMy
PRM
PR2
Laser
BS
ITMx
PR3
SR2
Mode matching
Alignment
Modulator
AOM
SR3
Beam shutter
Variable attenuator
EOPM
AOM
Laser
AOM
Laser
Reference Cavity
Mode cleaning
Phase lock
SRM
ETMx
II-1 Experiments
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Master laser frequency stabilization: absolute
frequency stabilization of NPRO (I2) & line-width
reduction by ULE (fiber) ring cavity (T. H. Yoon)
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Optical frequency comb metrology: Absolute long
distance measurement (T. H. Yoon)
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High power (> 200 W) fiber amplifier: Yb-doped
large-mode area photonic crystal fiber (Y.-H. Cha)
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Vibration isolation: Atomic interferometer (J. Kim)
Master Oscillator frequency stabilization
(T. H. Yoon, Korea Univ.)
NPRO
I2 spectrometer at
532 nm for absolute
frequency stabilization
Fiber ring cavity
Yb optical frequency comb metrology
(T. H. Yoon, Korea University)
976 nm
Pump laser
WDM
CFBG
OPL ~ 80.6 cm
YDF
AQWP
Chip PZT
R= 12.5 %
Beam block
7 W 915 nm
Pump laser
SESAM
1030 nm
R = 70 ~ 90 %
OI
Gain medium : YDF
Cavity components : CFBG, SESAM
Pump : 976 nm, single mode laser
All polarization maintaining fiber
Dispersion managed to be a positive value.
1030 nm
oscillator
0.1 W
915 nm
Pump/signal
combiner
Signal insertion
loss : 0.55 dB
Pump efficiency
:92.5 %
Double cladding YDF
t
= 2.8 ps
Pmax = 100 mW
frep = 186 MHz ~ 208 MHz
D = 26 nm
single polarization
Mirror
1040 nm
Transmission
grating pair
PCF
Yb optical frequency comb: Absolute long
distance metrology (T. H. Yoon)
PCF
fs Yb fiber comb
0
444 mW
27 mW
8
-20
Dt = 115.9 fs
b0 = 0
Powe (dBm)
Autocorrelation signal (a.u.)
-10
6
4
2
0
-400 -300 -200 -100
0
100
200
Delay (fs)
300
400
-30
-40
-50
-60
-70
-80
600 700 800 900 1000 1100 1200 1300 1400
Wavelength (nm)
S. Kim, Nat. Photon. 2010
High power Yb-doped fiber amplifier
(Y.-H. Cha, KAERI)
Structure of rod-type PCF
55 or 80 cm
Glass support
- f = 1.7 mm
- No outer coating
Pump clad, air gap
- f = 285 mm
- NA ~ 0.6
Signal core, Yb-doped, PM
- f = 100 mm, MFD = 76 mm
- NA ~ 0.02
- Pump absorption@ 976 nm
~ 30 dB/m (small signal)
End capped on both ends
- Material: fused silica
- Length: 8 mm
- Diameter: 8.2 mm
- AR coated
Yb-fiber MOPA system
- All fiber set-up
- Easy to handle
DFB
20 mW, 1056 nm
OI
Master Laser
LD
0.5 W
LD
5W
x
NPRO Nd:YAG
2m
x
x
Absolute frequency
AOM
stabilization
x
PM-SC
Yb by
Fiber
reduction
(6/125)
LD
25W
BPF
x
DL
Main Amplifier
(Rod-PCF)
x
Free Space
Coupling
O.I.
O.I. BPF
7m
3m
Line-width
ULE(or fiber) ring cavity
PM-DC
Yb Fiber
(5/130)
Pulse Generation &
Pre-Amplifier
PM-PCF
Yb Fiber
(40/200)
Mid-Amplifier
BPF
240
220
200
180
160
140
120
100
80
60
40
20
0
100
90
80
70
60
0
50
100
150
200
250
300
350
Pump absorption ratio (%)
Amplified output power(W)
Main amplifier with a rod PCF
-
- For 200 W cw laser
- Need to active research
Wavelength: 1056 nm
Repetition rate: 150 kHz
Max. amp. Power: 230 W (Ep = 1.5 mJ)
Pump absorption decreases at high-power
Max. SBS power: ~ 8 W at 230 W power
Pulse width: ~ 5 ns
SBS monitor
Absorbed Pump Power (W)
F=300 mm
NA: 0.22
Lens
Pump LD
- 976 nm
- 450 W
Isolator Isolator
Amplified
output
Transmitted
Pump
Rod PCF (80 cm)
SWP Lens
1056 nm
5-6 W (150 kHz)
Lens SWP
Vibration isolation: Atomic interferometer
(J. Kim, Myongji Univ.)
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Atomic gravimeter
AI is a good gravity sensor
Large dynamic range
No drift
2D-MOT
Earthquake
in 13 Jan.
2007
(Kuril Islands,
Mag.= 8.1)
seismometer
double
magnetic
shields
87Rb
L2 : repumper / Raman 1
L3 : cooling / Raman 2
σ+
σ-
Raman collimator
with adjustable /4
West 3D-MOT beam
East 3DMOT
beam
3D-MOT
detection
detection
σ-
σ+
λ/4
retro-reflection
mirror
isolation
platform
Vibration Rejection
PC
Seismometer
v(t) → fvibS
Interferometer
keffgT² + fvibS
Probabilité de transition
0.52
Sans correction
Avec correction
0.48
0.44
0.40
0.36
Nombre de coups
With correction : 1.4 10-8g @ 1 s
keffgT²
Post correction
Current Result & Problem
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Good agreement with tidal model
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Wave front aberration
Mirror
• 40 mm diameter
• PV= /10
• RMS =/100
Δg < 10-9 g with T = 2 µK
Long term stability comparable
to the accuracy of the tide model
4
10-10 g
 R > 10 km !
→ flatness
better than λ/300 !!!
Simulation :
• T = 2.5 mK
• s = 1.5 mm
g/g = 1.4 10-9
/4
g/g = 8 10-9
II-2 Data Analysis
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Quality Control
▶ Parameter Estimation for Compact Binary
Coalescence
▶ Fundamental research on gravitational wave
detection algorithm
▶ Optical Followup Data Analysis
▶ Mass processing of the data
II-3 Astrophysical and Theoretical
Research
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Optical followup observations using Korean
facilities
▶ Gravitational wave source related researches
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Binary formation and evolution in dense stellar systems
▶ Neutron star equation of states and binary evolution
▶ Pulsar glitch induced gravitational waves
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Others
Computational Resources @ GSDC-KISTI
KISTI has been providing largest computing resources
to Korean science community for about 40 years.
1,000,000
100,000
10,000
GFlops
360 TFlops
1,000
100
10
1
1988
1991
1994
1997
2000
Year
2003
2006
2009
Resource Allocation Plan for LSC and
LCGT
1. KISTI has dedicated computing facilities for Data Center Project, which
will include LIGO data analysis.
2. NIMS provides additional computing resources (currently 88 CPUs).
KISTI’s Plan for Data Center
Project
# of CPUs
Storage (TB)
2010
2011
2012
48
120 + 120
240+300
5
100
200
#120+120 means dedicated 120 and shared 120 cores
KISTI’s Data Center Team
• Ten staff members in engineering and computer
sciences (3 will work for LIGO data analysis)
• Experts in grid computing, installation and
software management for the data center
• Good network infrastructure, e.g. KREONET (20
Gbps) and GLORIAD (10 Gbps)
The KGWG and staff at KISTI will work with the UWM group in setting
up KISTI clusters in accordance with the LIGO Data Grid.
KMTNet (Korea Microlensing Telescope
Network)
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Three 2 m class telescopes will be built in South Africa, Chile, and Australia
for continuous coverage of microlensing events
To be fully operational in 2014
Optimized to detect time varying sources
KMTNet team is interested in collaboration with GW experiments for
coincidences & follow-ups
Primary Mirror
1.6 m
Focus
Prime Focus
Mosaic CCD
20k x 20k Mosaic CCD
FoV
2 deg x 2 deg
Permanent members (12 now, 15 next year)
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T. H. Yoon (Korea Univ.)
Leader of KGWG-LCGT Collaboration
Experimental: T. H. Yoon (Korea Univ.), J. Kim (MJU),
Y.-H. Cha (KAERI), to be joined next year [D. Cho
(Korea Univ.), H. S. Kang (APRI), J. M. Choi (CNU)]
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Data Analysis: H. W. Lee (Inje Univ.), H. M. Lee
(SNU), H. K. Lee (Hanyang Univ.), C.-H. Lee (PNU),
G. W. Kang (KISTI), J. Oh (NIMS), S. H. Oh (NIMS)
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Theoretical: M. G. Park (KPNU), S. P. Kim (Kunsan
National Univ.)
Summary
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KGWG will provide significant manpower and computing
resources for LCGT experiments, data analysis and
theoretical research
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Permanent Members = 12 (3 for experiment, 7 for data
analysis, and 2 for theory); possibly 15 next year (6 for
experiment)
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We are willing to expand our participation to wider area.
Any suggestions are welcome.